Acknowledgments for Collaboration: G. Mourou, C. Barty, W. Brocklesby, K. Nakajima, R. Hajima, T. Hayakawa, S. Gales, K. Homma, M. Kando, S. Bulanov, B. Holzer, T. Esirkepov, , F. Krausz, D. Habs, B. LeGarrec, J. Miquel, W. Leemans, D. Payne, P. Martin, R. Assmann, R. Heuer, M. Spiro, B. Holzer, W. Chou, M. Velasco, J.P. Koutchouk, M. Yoshida, T. Massard, G. Cohen-

Tannoudji, V. Zamfir, T. Ebisuzaki, R.X. Li, X. Q. Yan, K. Abazajian, S. Barwick, J. Limpert, D. Payne, K. Koyama, A. Suzuki, Y. Okada, K. Ishikawa, N. Rostoker

4th IZEST Conference

French Embassy, Tokyo

November 18, 2013

IZEST High Field Science: From Fundamental Physics

To Societal Applications

T. Tajima Norman Rostoker Professor, UCI

Deputy Director, IZEST

Guest Professor, KEK

content • High fields that break matter, but keep order

Guiding principle for order: not atomic cohesion (quantum

coherence), but relativistic coherence (and plasma’s collective

eigenmodes) (Lesson learned in N. Rostoker’s lab, 1973-75)

plasma acceleration, plasma decelerator, plasma optics,

plasma compressor, astrophysical acceleration,….

• High energy accelerators by laser

• Luminosity issue for collider---ICUIL-ICFA Joint Task

• Answer to high rep rate and high efficiency fiber laser (CAN)

• Laser (not charged particles) collider for Dark Fields search

• CAN lasers : enabling technology also for industrial and societal

applications: compact radiation oncology, directed gamma

beams (nuclear medicine and pharmacology), homeland security,

transmutation of nuclear wastes (ADS, etc.) , ….

High Field Science Supporters:

CERN

Rolf Heuer CERN Director General

New Paradigm PeV

TeV Standard Model Quarks Leptons

Extra dimension Dark matter Supersymmetry

Leptogenesis SUSY breaking

Atsuto Suzuki: KEK Director General,

Former ICFA Chair

IZEST’s Mission: Responding to Suzuki’s Challenge

Greetings from Michel Spiro (Former) President of CERN Council

As President of the CERN Council, I would like to express

our interest and warm support in developing new ultra high

gradient techniques of particle acceleration.

Plasma acceleration seems a very promising avenue.

The IZEST project is a bold and fierce adventure. It will

open the way to a new generation of ultra high energy

and compact accelerator and give access to totally new

physics like probing quantum vacuum and testing the

basic laws of physics.

I wish great success to the IZEST conference and to the

IZEST project.

Best wishes,

Michel

[Court. A. Oeftinger(CERN)]

______________________________ ___________________________________________

_________________________________________

(http://tesla.desy.de/~rasmus/media/Accelerator%20physics/slides/Livingston%20Plot%202.html)

Livingston Chart and Recent Saturation (S

uzu

ki, 2

00

9; fu

rthe

r co

rrecte

d 2

01

3)

→

→

ICUIL 2012 Mourou

Vacuum Polarization IZEST C3

Extreme Light Road Map

MeV

eV

MeV

GeV

TeV

J

MJ

kJ

mJ

Ep=mpc2

Ee=m0c2

LMJ/NIF, 2MJ, 3B€

ELI, kJ 0.3 B€

Brief History of ICUIL – ICFA Joint Effort – ICUIL Chair (Tajima) sounded on A. Wagner (Chair ICFA) and Suzuki

(incoming Chair) of a common interest in laser driven acceleration, Nov.

2008

– ICFA GA invited Tajima for presentation by ICUIL and endorsed initiation of

joint efforts on Feb. 13, 2009

– Joint Task Force formed of ICFA and ICUIL members, W. Leemans, Chair,

Sept, 2009

– First Workshop by Joint Task Force held @ GSI, Darmstadt, April, 2010

– Report to ICFA GA (July,2010) and ICUIL GA (Sept, 2010) on the findings

– EuroNNAc Workshop on Novel Accelerators (CERN, May, ’11)

– Publication of Joint Task Force Report (Dec. 2011)

– Start of ICAN Workshop Series @ CERN (Feb., 2012)

– US DOE AAC Workshop on advanced laser tech (2013)

– Final ICAN Conference @ CERN (June, 2013) next phase WE-CAN

Laser Wakefield (LWFA): nonlinear optics in plasma

Bow (‘ponderomotive’)

and Kelvin wake waves

Wave breaks at v＜c No wave breaks and wake peaks at v≈c

(The density cusps.

Cusp singularity)

(Plasma physics vs.

Superstring theory)

← relativity

regularizes (relativistic coherence)

cf: QCD wake/bow (Chesler/Yaffe 2008):

Maldacena (string theory) method

Hokusai

Maldacena

Laser driven collider concept

High-density design (Xie,97; Leemans,09)

ICFA-ICUIL Joint Task Force on Laser Acceleration(Darmstadt,10)

a TeV collider

Laser energy: UL ~ n0-3/2

Total wall plug power (Low-density Nakajima: Pwall ~ n0

3/2 )

21

0nPNP avgstagewall

100 GeV (~Higgs energy) ascent: Challenging! Inspirational Needs international teamwork!

Please join us!

Nakajima, LeGarrec

First Workshop on 100GeV IZEST Project: May 31-June 1, ’12 @ Bordeaux

Courtesy of PETAL

Nakajima

IZEST 100GeV Ascent

1GeV

100GeV-PETAL 2015

1TeV-PETAL/LMJ

10GeV-GSI/SIOM/// 2013

16

Den

sity scalings o

f LWFA

fo

r collid

er

_______________________ _____

(Nakajima, PR STAB, 2011) 1018 /cc (conventional) → 1016 /cc

_________________________________________ _________

2 2 2 2 2

0 0 0 02 2 ,crph

e

nE m c a m c a

n

2

0

2,cr

d p

e

nL a

n

0

1,

3

crp p

e

nL a

n

(when 1D theory applies)

Theory of wakefield toward extreme energy

In order to avoid wavebreak,

a0 < γph1/2 ,

where

γph = (ncr / ne )1/2

100

101

102

103

104

105

106

107

Ele

ctr

on e

nerg

y (

MeV

)

1017

1018

1019

1020

Plasma density (cm-3)

1 GeV

1 TeV

dephasing length pump depletion length

Adopt:

NIF laser (3MJ)

→ 0.7PeV (with Kando, Teshima)

←experimental

←theoretical

18

Einstein and Ether

(A. Einstein, 1922)

_____________________________________________________________________________

Feel vacuum texture: PeV energy γ

PeV γ (converted from e- )

←(1PeV : fs behind)

← (0.1PeV)

1km

Laser acceleration → controlled laboratory test to see quantum gravity texture

on photon propagation (Special Theory of Relativity: c0)

Coarser,

lower energy

texture

Finer,

higher energy

texture

c < c0

γ-ray signal from primordial GRB

Energy-dependent

photon speed ?

Observation of primordial

Gamma Ray Bursts (GRB)

(limit is pushed up

close to Planck mass)

Lab PeV γ (from e-)

can explore this

with control

(Abdo

, et al, 200

9)

←lo

wer e

nerg

y h

igher →

Etat de l’Art (HEEAUP 2005): collider consideration

LIL

1 J

1 k J

100 J

10 J

10 k J

100 k J

1 M J

10 M J

0,1 J

LULI

LMJ/NIF

10 2 10 1 10 -1

10 -2

10 -3

10 -4

10 -5

LULI 100TW

Commercial

LULI 2000

pico 2000

Taux de répetition (Hz)

100J/10Hz Luli

150J/.1Hz

Jena

104

Laser Fusion 15MW Linear Accelerator

100MW

Mourou (2005)

Mourou/ICAN (2013); Nakajima (2011)

IZEST (International Center for Zetta- Exawatt Science and Technology)

aspires to push the average power

of ultraintense laser from Watt to MW

(ICAN-International Coherent Amplification Network)

polar.

controller

1W PM

EDFAs

16 × 4-channels PLZT

phase modulators far-field

observation

laser output

Phase processing and

feedback loop

1×2 splitters

1×16 splitters

1W PM EDFA

Laser

diode

1.55µm

2:1image relay

fiber

array

lenslet

array

QWLSI

J. Bourderionnet, A. Brignon (Thales), C. Bellanger, J. Primot (ONERA)

Coherent Fiber Combining

Achievement 2011

64 phase-locked fibers

ICUIL 2012 Mourou

ICUIL 2012 Mourou

Opportunities Enabled by CAN

CAN Fiber Laser Collider requirements Average power luminosity rep rate x peak power Efficiency cost Smartness (digital control) emittance Intensity gradient

γ-γ collider requirements 1-50kHz rep rate (other reqs are easier)

Dark matter search average power luminosity

Proton acceleration intensity (energy of beam), smartness

(beam quality), average power (fluence)

R. A

leks

an (C

ou

rt. A

. Oef

tin

ger(

CER

N))

(γγ collider) (W. Chou et al.)

M. Velasco (Court. A. Oeftinger)

27

Beyond QED photon-photon interaction

√ｇ

√ｇ

M-1

mass m

M-1

√ｇ

√ｇ

FFgM 1

FFgM~1

Resonance in quasi-parallel collisions in low cms energy

If M~MPlanck, Dark Energy

QCD-instanton, Dark Matter

])~

(7)(4[360

1 222

4

FFFF

mLQED

Away from 4 : 7 = QCD , low-mass scalar , or pseudoscalar (unlike Higgs, which is heavy fields for photon-photon interaction,)

FFFF

~

K.Homma, D.Habs, T.Tajima (2011)

arXiv:1006.1762 [gr-qc] Y. Fujii and K.Homma

Quantum anomaly

e.g. xw 1w

Degenerate Four-Wave Mixing (DFWM)

Decay into (4-x)ω can be induced by frequency-mixing

.

28

K.Homma, D.Habs, T.Tajima Appl. Phys. B (2011)

Laser-induced nonlinear optics in vacuum (cf. Nonlinear optics in crystal)

Wirth et al. (Science 2011: synthesized light transients)

Sweep by arbitrary frequency xw

Photon mixer’s road to unknown fields: Dark Matter and Dark Energy

29

Log

g/M

[1

/Ge

V]

K.Homma, D.Habs, T.Tajima (2011)

(Court. A. Oeftinger)

Mountain of Radioactive Junk at Nuclear Facility

B. Carluec (Court. A. Oeftinger(CERN))

Sharp discriminatory capability of monoenergetic gamma rays

vs

Bremsstrahlung gamma rays Laser Compton gamma rays

C. Barty and T. Tajima (2008)

Nu

clear Reso

nan

ce fluo

rescence sign

al

Brilliance of Laser Compton gamma source

Barty an

d Tajim

a, 20

08

10GeV-TeV proton Energy Scalings(RPA x LWFA ) TeV over cm @ 1023W/cm2 (Zheng et al, 2012) 10GeV over mm @ 1022W/cm2 (Zheng et al, 2013)

200MeV @1021W/cm2 (Wang et al, 2013)

ICUIL 2012 Mourou

Extreme High Energy Cosmic Rays (EHECR)

AMS Launch

May 16, 2011

JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module

~ 4 ~

JEUSO-110025-01-E-TR-ZZZ

since the mean distance to EAS and atmospheric absorption both increase. First few years of the

then later to

Figure 1-2. Artistic illustration of the JEM-EUSO telescope attached to the Japanese Experiment Module of the International Space Station, under nadir (left) and tilt (right) mode of observation.

The JEM-EUSO telescope can reconstruct the incoming direction of the EECRs with accuracy

better than few degrees. Its observational aperture of the ground area is a circle with 250 km

radius, and its atmospheric volume above it, with a 60° FoV, is ~1 Tera-ton or more. The target

volume for upward neutrino events exceeds 10 Tera-tons. The instantaneous aperture of JEM-

EUSO is larger than the Pierre Auger Southern Observatory by a factor ranging from 65 to 280,

depending on its observation mode (nadir or tilted, Fig.1-3).

JEM-EUSO, planned to be attached to JEM/EF of ISS, will be launched in the JFY 2016 by

H2B rocket and conveyed to ISS by HTV (H-II transfer Vehicle).

Figure 1-3. Area observed by the JEM-EUSO telescope in one shot under mode.

ISS-CREAM

Sp-X Launch 2014

JEM-EUSO

Launch Tentatively

planned for 2017

CALET on JEM

HTV Launch 2014

JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module

~ 4 ~

JEUSO-110025-01-E-TR-ZZZ

since the mean distance to EAS and atmospheric absorption both increase. First few years of the

then later to

Figure 1-2. Artistic illustration of the JEM-EUSO telescope attached to the Japanese Experiment Module of the International Space Station, under nadir (left) and tilt (right) mode of observation.

The JEM-EUSO telescope can reconstruct the incoming direction of the EECRs with accuracy

better than few degrees. Its observational aperture of the ground area is a circle with 250 km

radius, and its atmospheric volume above it, with a 60° FoV, is ~1 Tera-ton or more. The target

volume for upward neutrino events exceeds 10 Tera-tons. The instantaneous aperture of JEM-

EUSO is larger than the Pierre Auger Southern Observatory by a factor ranging from 65 to 280,

depending on its observation mode (nadir or tilted, Fig.1-3).

JEM-EUSO, planned to be attached to JEM/EF of ISS, will be launched in the JFY 2016 by

H2B rocket and conveyed to ISS by HTV (H-II transfer Vehicle).

Figure 1-3. Area observed by the JEM-EUSO telescope in one shot under mode.

ISS-CREAM

Sp-X Launch 2014

JEM-EUSO

Launch Tentatively

planned for 2017 Adapted from Simpson 1983 in PDG by M. Casolino

LHC

PAMELA

35

Cen A: an example of AGN • Distance：3.4Mpc

• Radio Galaxy

– Nearest

– Brightest radio source

(collective oscillations!)

• Elliptical Galaxy

• Disk, AGN jets, halos:

visible

• Other AGN: similar

Optical

Brightest AGNs

Conclusions High field science frontier expanding Laser-driven accelerators for high energy physics collider in particular Large fluence, high efficiency of CAN lasers important for many new scientific and societal applications CAN laser = smart laser : highly controllable Higgs factory by γ-γ collider emerging New weak-coupling field search of vacuum by laser Nuclear transmutation by laser-driven neutron sources, ADS, ADR; compact neutrino source Non-contact detection of nuclear isotopes via laser Compton gamma rays (Fukushima) Other industrial applications (auto-industry, chemical

industry, mechanical industry, medical, etc.) with large fluence and high efficiency lasers

EHECR <--> terrestrial laser acceleration

Blazar: Cosmic laser wakefield linac?

ありがとうございます!